The luminosity function of field galaxies and its evolution 
  since $\vec{z=1}$

Fried, J. W.; Kuhlmann, B. von; Meisenheimer, K.; Rix, H. W.; Wolf, Christian; Hippelein, H.; Kümmel, M.; Phleps, S.; Röser, H.-J.; Thierring, I.; Maier, C.

doi:10.1051/0004-6361:20000466

Cited by 39 publications

(90 citation statements)

References 28 publications

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“…This noevolution assumption is usually justified by appealing to results from galaxy number counts ( Im et al 2002;Schade et al 1999) and the redshift distribution of lens galaxies (Ofek et al 2003), which are consistent with the hypothesis that the early-type population evolves only through passive luminosity evolution. However, the observational status of early-type evolution has been controversial (Lin et al 1999;Kauffmann et al 1996;Totani & Yoshii 1998;Fried et al 2001), and the observational uncertainties are large enough that dynamical number or mass evolution in the early-type galaxy population cannot be ruled out.…”

Section: A Model For Redshift Evv Olution Of the Lens Populationmentioning

confidence: 99%

Improved Cosmological Constraints from Gravitational Lens Statistics

Mitchell¹,

Keeton²,

Frieman³

et al. 2005

ApJ

133

238

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We combine the Cosmic Lens All-Sky Survey (CLASS) with new Sloan Digital Sky Survey (SDSS) data on the local velocity dispersion distribution function of E /S0 galaxies, ( ), to derive lens statistics constraints on Ã and m . Previous studies of this kind relied on a combination of the E /S0 galaxy luminosity function and the FaberJackson relation to characterize the lens galaxy population. However, ignoring dispersion in the Faber-Jackson relation leads to a biased estimate of ( ) and therefore biased and overconfident constraints on the cosmological parameters. The measured velocity dispersion function from a large sample of E/S0 galaxies provides a more reliable method for probing cosmology with strong lens statistics. Our new constraints are in good agreement with recent results from the redshift-magnitude relation of Type Ia supernovae. Adopting the traditional assumption that the E/S0 velocity function is constant in comoving units, we find a maximum likelihood estimate of Ã ¼ 0:74 0:78 for a spatially flat universe (where the range reflects uncertainty in the number of E/S0 lenses in the CLASS sample) and a 95% confidence upper bound of Ã < 0:86. If ( ) instead evolves in accord with the extended PressSchechter theory, then the maximum likelihood estimate for Ã becomes 0.72-0.78, with the 95% confidence upper bound Ã < 0:89. Even without assuming flatness, lensing provides independent confirmation of the evidence from Type Ia supernovae for a nonzero dark energy component in the universe.

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Section: A Model For Redshift Evv Olution Of the Lens Populationmentioning

confidence: 99%

Improved Cosmological Constraints from Gravitational Lens Statistics

Mitchell¹,

Keeton²,

Frieman³

et al. 2005

ApJ

133

238

View full text Add to dashboard Cite

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“…The CADIS (Fried et al 2001) and COMBO-17 (Wolf et al 2003) surveys, based on photometric redshifts using medium-band filters, also provide consistent intrinsic LFs in the B band with the CNOC2 and ESO-Sculptor. The 4 mentioned surveys are based on CCD photometry combined with a spectral classification with accurate flux calibration, which therefore appears, among the mentioned surveys, as the optimal combination for estimating the intrinsic LFs.…”

Section: Conclusion and Prospectsmentioning

confidence: 66%

“…Both the CADIS and CFRS measure LFs in the intervals 0.5 < ∼ z < ∼ 0.75 and 0.75 < ∼ z < ∼ 1.0, in which they detect evolutionary effects using the LFs with z ≤ 0.5 as reference. I however use their intrinsic LFs derived in the intervals 0.3 ≤ z ≤ 0.5 and 0.2 ≤ z ≤ 0.5 resp., because these provide the best constraint on α for each survey (see Fried et al 2001;Lilly et al 1995); these redshift intervals also correspond to z max < ∼ 0.6. For the CFRS, the values of M * , listed for h = 0.5 (Lilly et al 1995), are converted to h = 1.…”

Section: B Luminosity Functions At Redshifts 04-06mentioning

confidence: 98%

“…Note that here, the denomination "redshift survey" means "systematic survey of a region of the sky wide enough to include both cluster/group galaxies and field galaxies, and for which estimates of redshifts are provided". I therefore include the surveys by Fried et al (2001) and Wolf et al (2003), based on medium-band photometric redshifts; both surveys provide useful estimates of intrinsic LFs, consistent with those from the other surveys in the B band, which a posteriori justifies their inclusion into the analysis.…”

Section: Introductionmentioning

confidence: 96%

“…The recent morphological analysis of a sub-sample of the Sloan Digital Sky Survey (Nakamura et al 2003) based on CCD imaging to z ∼ 0.1 however shows evidence for a contribution from dwarf galaxies. At redshifts larger than ∼0.1, visual morphological classification becomes highly uncertain and is replaced by spectral classification (Heyl et al 1997;Bromley et al 1998;Lin et al 1999;Folkes et al 1999;Fried et al 2001;Madgwick et al 2002;Wolf et al 2003;de Lapparent et al 2003b). Other redshifts surveys for which a spectral classification is not available use either colors (Lilly et al 1995;Lin et al 1997;Metcalfe et al 1998;Brown et al 2001) or the strength of the emission lines (Lin et al 1996;Small et al 1997;Zucca et al 1997;Loveday et al 1999) for estimating the LFs of the different galaxy types.…”

Section: Introductionmentioning

confidence: 99%

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Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

Lapparent

2003

A&A

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Abstract. I perform a quantitative comparison of the shape of the optical luminosity functions as a function of galaxy class and filter, which have been obtained from redshift surveys with an effective depth ranging from z 0.01 to z 0.6. This analysis is based on the M * and α Schechter parameters which are systematically measured for all galaxy redshift surveys. I provide complete tables of all the existing measurements, which I have converted into the UBVR c I c Johnson-Cousins system wherever necessary.By using as reference the intrinsic luminosity functions per morphological type, I establish that the variations in the luminosity functions from survey to survey and among the galaxy classes are closely related to the criteria for galaxy classification used in the surveys, as these determine the amount of mixing of the known morphological types within a given class. When using a spectral classification, the effect can be acute in the case of inaccurate spectrophotometric calibrations: the luminosity functions are then biased by type contamination and display a smooth variation from type to type which might be poorly related to the intrinsic luminosity functions per morphological type. In the case of surveys using multi-fiber spectroscopy, galaxy classification based on rest-frame colors might provide better estimates of the intrinsic luminosity functions.It is noticeable that all the existing redshift surveys fail to measure the Gaussian luminosity function for Spiral galaxies, presumably due to contamination by dwarf galaxies. Most existing redshift surveys based on visual morphological classification also appear to have their Elliptical/Lenticular luminosity functions contaminated by dwarf galaxies. In contrast, the analyses using a reliable spectral classification based on multi-slit spectroscopy or medium-filter spectrophotometry, and combined with accurate CCD photometry succeed in measuring the Gaussian luminosity function for E/S0 galaxies. The present analysis therefore calls for a more coherent approach in separating the relevant giant and dwarf galaxy types, a necessary step towards measuring reliable intrinsic luminosity functions.

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The Assembly of Present‐Day Galaxies as Witnessed by Deep Surveys

Meisenheimer

2008

Reviews in Modern Astronomy

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The luminosity function of field galaxies and its evolution since $\vec{z=1}$

Cited by 39 publications

References 28 publications

Improved Cosmological Constraints from Gravitational Lens Statistics

Improved Cosmological Constraints from Gravitational Lens Statistics

Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

The Assembly of Present‐Day Galaxies as Witnessed by Deep Surveys

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